The Formation and Early Evolution of Star Clusters

10.1142/p764 ◽  
2022 ◽  
Author(s):  
Simon Goodwin ◽  
Nate Bastian
Keyword(s):  
Star Clusters ◽  
Early Evolution

scholarly journals The early evolution of star clusters in compressive and extensive tidal fields

2017 ◽  
Vol 468 (1) ◽  
pp. L92-L96 ◽  
Author(s):  
Jeremy J. Webb ◽  
Saahil S. Patel ◽  
Enrico Vesperini
Keyword(s):  
Star Clusters ◽  
Early Evolution

scholarly journals On the early evolution of massive star clusters: the case of cloud D1 and its embedded cluster in NGC 5253

2020 ◽  
Vol 494 (1) ◽  
pp. 97-107 ◽  
Author(s):  
Sergiy Silich ◽  
Guillermo Tenorio-Tagle ◽  
Sergio Martínez-González ◽  
Jean Turner
Keyword(s):  
Massive Star ◽  
Massive Stars ◽  
Star Clusters ◽  
Early Evolution ◽  
Mass Loading ◽  
Low Mass Stars ◽  
Stellar Cluster ◽  
Star Forming ◽  
Cluster Phase ◽  
Protostellar Discs

ABSTRACT We discuss a theoretical model for the early evolution of massive star clusters and confront it with the ALMA, radio, and infrared observations of the young stellar cluster highly obscured by the molecular cloud D1 in the nearby dwarf spheroidal galaxy NGC 5253. We show that a large turbulent pressure in the central zones of D1 cluster may cause individual wind-blown bubbles to reach pressure confinement before encountering their neighbours. In this case, stellar winds energy is added to the hot shocked wind pockets of gas around individual massive stars that leads them to meet and produce a cluster wind in time-scales less than 105 yr. In order to inhibit the possibility of cloud dispersal, or the early negative star formation feedback, one should account for mass loading that may come, for example, from pre-main-sequence (PMS) low-mass stars through photoevaporation of their protostellar discs. Mass loading at a rate in excess of 8 × 10−9 M⊙ yr−1 per each PMS star is required to extend the hidden star cluster phase in this particular cluster. In this regime, the parental cloud remains relatively unperturbed, while pockets of molecular, photoionized and hot gas coexist within the star-forming region. Nevertheless, the most likely scenario for cloud D1 and its embedded cluster is that the hot shocked winds around individual massive stars should merge at an age of a few million of years when the PMS star protostellar discs vanish and mass loading ceases that allows a cluster to form a global wind.

scholarly journals Pre-Collapse Evolution of Galactic Globular Clusters

1996 ◽  
Vol 174 ◽  
pp. 365-366
Author(s):  
Toshiyuki Fukushige ◽  
Douglas C. Heggie
Keyword(s):  
Mass Spectrum ◽  
Mass Loss ◽  
Stellar Evolution ◽  
Globular Clusters ◽  
Star Clusters ◽  
Early Evolution ◽  
Initial Structure ◽  
Spherically Symmetric ◽  
Order Of Magnitude ◽  
Model Star

We investigated collisionless aspects of the early evolution of model star clusters. The effects of mass loss through stellar evolution and of a steady tidal field are modelled using N-body simulations. Our results (which depend on the assumed initial structure and the mass spectrum) agree qualitatively with those of Chernoff & Weinberg (1990), who used a Fokker-Planck model with a spherically symmetric tidal cutoff. For those systems which are disrupted, the lifetime to disruption generally exceeds that found by Chernoff & Weinberg, sometimes by as much as an order of magnitude.

scholarly journals From hydrodynamics to N-body simulations of star clusters: mergers and rotation

2020 ◽  
Author(s):  
Alessandro Ballone ◽  
Stefano Torniamenti ◽  
Michela Mapelli ◽  
Ugo N Di Carlo ◽  
Mario Spera ◽  
...  
Keyword(s):  
Initial Conditions ◽  
Star Clusters ◽  
Mass Function ◽  
Young Star ◽  
Initial Mass Function ◽  
Early Evolution ◽  
Stellar Feedback ◽  
Gas Removal ◽  
Hydrodynamical Simulations ◽  
Young Star Clusters

Abstract We present a new method to obtain more realistic initial conditions for N-body simulations of young star clusters. We start from the outputs of hydrodynamical simulations of molecular cloud collapse, in which star formation is modelled with sink particles. In our approach, we instantaneously remove gas from these hydrodynamical simulation outputs to mock the end of the gas-embedded phase, induced by stellar feedback. We then enforce a realistic initial mass function by splitting or joining the sink particles based on their mass and position. Such initial conditions contain more consistent information on the spatial distribution and the kinematical and dynamical states of young star clusters, which are fundamental to properly study these systems. For example, by applying our method to a set of previously run hydrodynamical simulations, we found that the early evolution of young star clusters is affected by gas removal and by the early dry merging of sub-structures. This early evolution can either quickly erase the rotation acquired by our (sub-)clusters in their embedded phase or “fuel” it by feeding of angular momentum by sub-structure mergers, before two-body relaxation acts on longer timescales.

scholarly journals The effects of a background potential in star cluster evolution

2020 ◽  
Vol 639 ◽  
pp. A92 ◽  
Author(s):  
B. Reinoso ◽  
D. R. G. Schleicher ◽  
M. Fellhauer ◽  
N. W. C. Leigh ◽  
R. S. Klessen
Keyword(s):  
Binary Stars ◽  
Gravitational Force ◽  
Massive Star ◽  
Star Clusters ◽  
Star Cluster ◽  
Early Evolution ◽  
Relaxation Processes ◽  
Blue Stragglers ◽  
Stellar Collisions ◽  
The Universe

Runaway stellar collisions in dense star clusters are invoked to explain the presence of very massive stars or blue stragglers in the center of those systems. This process has also been explored for the first star clusters in the Universe and shown to yield stars that may collapse at some points into an intermediate mass black hole. Although the early evolution of star clusters requires the explicit modeling of the gas out of which the stars form, these calculations would be extremely time-consuming and often the effects of the gas can be accurately treated by including a background potential to account for the extra gravitational force. We apply this approximation to model the early evolution of the first dense star clusters formed in the Universe by performing N-body simulations, our goal is to understand how the additional gravitational force affects the growth of a very massive star through stellar mergers in the central parts of the star cluster. Our results show that the background potential increases the velocities of the stars, causing an overall delay in the evolution of the clusters and in the runaway growth of a massive star at the center. The population of binary stars is lower due to the increased kinetic energy of the stars, initially reducing the number of stellar collisions, and we show that relaxation processes are also affected. Despite these effects, the external potential enhances the mass of the merger product by a factor ∼2 if the collisions are maintained for long times.

scholarly journals Contribution of globular clusters to halos

2015 ◽  
Vol 12 (S316) ◽  
pp. 287-293
Author(s):  
Angela Bragaglia
Keyword(s):  
Star Formation ◽  
Formation Mechanism ◽  
Globular Clusters ◽  
Massive Star ◽  
Milky Way ◽  
Star Clusters ◽  
Early Evolution ◽  
Light Elements ◽  
Halo Stars ◽  
Chemical Signatures

AbstractThe contribution of massive star clusters to their hosting halo dramatically depends on their formation mechanism and their early evolution. Massive globular clusters in the Milky Way (and in other galaxies) have been shown to display peculiar chemical patterns (light-elements correlations and anti-correlations) indicative of a complex star formation, confirmed by photometric evidence (spread or split sequences). I use these chemical signatures to try to understand what is the fraction of halo stars originally born in globular clusters.

scholarly journals Dynamics of Planetary Systems within Star Clusters: Aspects of the Solar System’s Early Evolution

2020 ◽  
Vol 159 (3) ◽  
pp. 101 ◽  
Author(s):  
Konstantin Batygin ◽  
Fred C. Adams ◽  
Yuri K. Batygin ◽  
Erik A. Petigura
Keyword(s):  
Star Clusters ◽  
Planetary Systems ◽  
Early Evolution

scholarly journals Super Hot Cores in NGC 253: witnessing the formation and early evolution of super star clusters

2019 ◽  
Vol 491 (3) ◽  
pp. 4573-4589 ◽  
Author(s):  
F Rico-Villas ◽  
J Martín-Pintado ◽  
E González-Alfonso ◽  
S Martín ◽  
V M Rivilla
Keyword(s):  
Star Formation ◽  
Uv Radiation ◽  
Star Clusters ◽  
Early Evolution ◽  
Evolutionary Stage ◽  
Vibrationally Excited ◽  
The Galaxy ◽  
Order Of Magnitude ◽  
Super Star Clusters ◽  
Inside Out

ABSTRACT Using 0.2 arcsec (∼3 pc) ALMA images of vibrationally excited HC3N emission (HC3N*) we reveal the presence of eight unresolved Super Hot Cores (SHCs) in the inner 160 pc of NGC 253. Our LTE and non-LTE modelling of the HC3N* emission indicate that SHCs have dust temperatures of 200–375 K, relatively high H2 densities of (1−6) × 106 cm−3 and high IR luminosities of (0.1–1) × 108 L⊙. As expected from their short-lived phase (∼104 yr), all SHCs are associated with young super star clusters (SSCs). We use the ratio of luminosities from the SHCs (protostar phase) and from the free–free emission (ZAMS star phase), to establish the evolutionary stage of the SSCs. The youngest SSCs, with the larges ratios, have ages of a few 104 yr (proto-SSCs) and the more evolved SSCs are likely between 105 and 106 yr (ZAMS-SSCs). The different evolutionary stages of the SSCs are also supported by the radiative feedback from the UV radiation as traced by the HNCO/CS ratio, with this ratio being systematically higher in the young proto-SSCs than in the older ZAMS-SSCs. We also estimate the SFR and the SFE of the SSCs. The trend found in the estimated SFE ($\sim 40{{\ \rm per\ cent}}$ for proto-SSCs and $\gt 85{{\ \rm per\ cent}}$ for ZAMS-SSCs) and in the gas mass reservoir available for star formation, one order of magnitude higher for proto-SSCs, suggests that star formation is still going on in proto-SSCs. We also find that the most evolved SSCs are located, in projection, closer to the centre of the galaxy than the younger proto-SSCs, indicating an inside-out SSC formation scenario.

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